wvrgcal_pg.wvrgcal_pg_ Class Reference

List of all members.

Public Member Functions
def	__init__
def	__call__
Private Attributes
	__bases__
	__doc__
Static Private Attributes
string	__name__

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Detailed Description

Definition at line 18 of file wvrgcal_pg.py.

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Constructor & Destructor Documentation

def wvrgcal_pg.wvrgcal_pg_.__init__

(

self

)

Definition at line 21 of file wvrgcal_pg.py.

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Member Function Documentation

def wvrgcal_pg.wvrgcal_pg_.__call__	(		self,
			vis = None,
			caltable = None,
			toffset = None,
			segsource = None,
			sourceflag = None,
			tie = None,
			nsol = None,
			disperse = None,
			wvrflag = None,
			statfield = None,
			statsource = None,
			smooth = None,
			scale = None,
			reversespw = None,
			cont = None,
			async = None
	)

Generate a gain table based on Water Vapour Radiometer data

Information about the observation and the performance of WVRGCAL is written to the CASA logger; 
see the CASA cookbook for a more detailed description of these parameters.

Of particular note is the discrepancy parameter (Disc): high values (> a few hundred microns) 
may indicate some levels of cloud contamination and the effect of applying the WVRGCAL correction 
should be checked; values > 1000 um in all antennas have currently been found to indicate that 
WVRGCAL correction should not be used.

      
  vis -- Name of input visibility file
      default: none; example: vis='ngc5921.ms'

  caltable -- Name of output gain calibration table
      default: none; example: caltable='ngc5921.wvr'

  toffset -- Time offset (sec) between interferometric and WVR data
     default: -1 (ALMA default)

  segsource -- Do a new coefficient calculation for each source
     default: True

  tie -- Prioritise tieing the phase of these sources as well as possible
 (requires segsource=True)
     default: [] example: ['3C273,NGC253', 'IC433,3C279']

  sourceflag -- Flag the WVR data for these source(s) as bad and do not produce corrections for it
       (requires segsource=True)
       default: [] (none) example: ['3C273']

  nsol -- Number of solutions for phase correction coefficients during this observation.
  By default only one set of coefficients is generated for the entire observation. 
  If more sets are requested, then they will be evenly distributed in time throughout 
  the observation. Values > 1 require segsource=False.
     default: 1

  disperse -- Apply correction for dispersion
     default: False

  wvrflag -- Flag the WVR data for these antenna(s) as bad and replace its data with interpolated values
       default: [] (none) example: ['DV03','DA05','PM02']           

  statfield -- Compute the statistics (Phase RMS, Disc) on this field only
       default: '' (all) 

  statsource -- Compute the statistics (Phase RMS, Disc) on this source only
       default: '' (all)             

  smooth -- Smooth WVR data by this many samples before applying the correction
     default: 1 (no smoothing) example: 3

  scale -- Scale the entire phase correction by this factor
     default: 1. (no scaling)

  reversespw -- Reverse the sign of the correction for the listed SPWs
(only neede for early ALMA data before Cycle 0)
     default: '' (none), example: reversespw='0~2,4'; spectral windows 0,1,2,4

  cont -- Estimate the continuum (e.g., due to clouds)
     default: False

Definition at line 26 of file wvrgcal_pg.py.

References vla_uvfits_line_sf.verify.

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Member Data Documentation

wvrgcal_pg.wvrgcal_pg_.__bases__ [private]

Definition at line 22 of file wvrgcal_pg.py.

wvrgcal_pg.wvrgcal_pg_.__doc__ [private]

Definition at line 23 of file wvrgcal_pg.py.

string wvrgcal_pg.wvrgcal_pg_.__name__ [static, private]

Definition at line 19 of file wvrgcal_pg.py.

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The documentation for this class was generated from the following file:

• wvrgcal_pg.py